The Konus-FG cosmic gamma-ray burst experiment for GAMMA-400 ...

The Konus-FG cosmic gamma-ray burst experiment for GAMMA-400 ...

The Konus-FG experiment for gamma-ray burst studies in GAMMA-400 M.V. Ulanov, R.L. Aptekar, D.D. Frederiks, S.V. Golenetskii, E.P. Mazets, and V.D. Palshin Ioffe Physical-Technical Institute, St. Petersburg, Russia Historical remarks GRB research experiments:

KONUS / Venera 1114 (19791983) KONUS-WIND (1994present time) CORONAS-I, CORONAS-F, CORONASPHOTON (20012009) Autonomous localization: GRANAT (1989) KONUS-A / Cosmos-2326, 2367, 2421 (19952008) Joint Russian-American Konus-Wind experiment

WIND 1994present time WIND orbit Konus-Wind GRB Experiment Two detectors S1 and S2 (NaI(Tl) 13cm

diameter, 7.5cm height, Be entrance window). Placed on opposite faces of the spacecraft, observing the south and north ecliptic hemispheres of the sky. Background mode: G1 (2080 keV), G2 (80300 keV), G3 (3001200 keV) with time resolution 1.472.94 sec.

Burst mode: time resolution 2ms256ms, energy spectra (20keV15MeV). Scientific goals of the Konus-FG experiment

Detection and prompt (12 sec) localization of GRB sources in 10 keV 3 MeV energy range with accuracy of 0.53. Localization information can be used for GAMMA-400 pointing to burst source or for further data analysis.

Study of temporal and spectral properties in 10 keV 15 MeV range with two highsensitive spectrometers. Schematic diagram of the Konus-FG instrument Spectrometers

Localization array of four detectors with anisotropic sensitivity Konus-FG-DN: localization units The localization subsystem is formed by four identical detectors Konus-FG-DN, registering photons in 10700 keV range. The detectors anisotropic angular sensitivity is

proportional to the cosine of the angle of incidence and is formed in the soft part of spectrum ~40 160 keV. The axes of the DNs are offset from the symmetry axis by 30 and separated in azimuth by 90. Field of view of each detector (2 sr) should not be occulted by construction details of the telescope. The system provides burst localization in upper hemisphere within detectors field of view (~75% of 2 sr) that exceeds the effective angular aperture of

the telescope. Konus-FG-DS: spectrometry units The spectrometric subsystem includes two identical wide directional spectrometry detectors Konus-FGDS operating in 10keV15MeV energy range. The axis of the detectors should be pointed parallel to the main spacecraft axis that provides the survey of the whole celestial sphere 4 sr. DS detectors obtain detailed information about energy spectra and time history of bursts.

Konus-FG-DS will be a valuable part of triangulation network (IPN), which will improve the reliability and accuracy of automatic localization. Location of Konus-FG units (preliminary) Konus-FG-DN Konus-FG-DS Konus-FG-DN

The Konus-FG-DS detector unit The main parts of the detector: 1 NaI(Tl) crystal 5 in diameter by 3 in height, 2 beryllium entrance window, 4 lead glass, 6 photomultiplier, 12, 13, 14 electronic boards . The Konus-FG-DN detector unit The main parts of the detector: 1 NaI(Tl) crystal 5 in diameter by 1 in height, 2 beryllium entrance window, 3 lead shield, 4 lead glass, 6 photomultiplier, 12, 13, 14 electronic boards .

Konus-A / Cosmos 2326, 2367 Localization detector prototype Each detector had 130 mm in diameter and 30 mm in height

with the passive shielding on lateral side. The axes of detectors are offset from symmetry axis by 30 and separated in azimuth by 90 . The accuracy of localization is of 0.5 to 23 angular degrees depending on the burst intensity.

R.L.Aptekar et al. ApJ 1998, 493, 404-407 Unsolved problems Arrangement the optimal location of Konus-FG detectors on the GAMMA-400

spacecraft. Broadband observations of the naked-eye gamma-ray burst GRB080319B The ultra-luminous GRB110918A Konus-Wind and Helicon (CORONAS-F) simultaneous observations of giant flare from SGR1806-20 on December 27, 2004

Konus-Wind and Helicon (CORONAS-F) simultaneous observations of giant flare from SGR1806-20 on December 27, 2004 The full isotropic energy release Q=2,31046 erg and the peak luminosity L=3,51047 -1 (Frederiks et al., Astronomy Lett., 2007)

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